1. ACTIVE GALAXIES and GALAXY EVOLUTION
Quasars,
Radio Galaxies,
Seyfert Galaxies and
BL Lacertae Objects
Immense powers emerging from ACTIVE GALACTIC NUCLEI:
it’s just a phase they’re going through!

2. How do we observe the life histories of galaxies?

3. Deep observations show us very distant galaxies as they were much earlier in time
(Old light from young galaxies)

6. How did galaxies form?

7. We still can’t directly observe the earliest galaxies

8. Our best models for galaxy formation assume:
Matter originally
filled all of space
almost uniformly
Gravity of denser
regions pulled in
surrounding
matter

9. Denser regions contracted, forming protogalactic clouds
H and He gases in these clouds formed the first stars

10. Supernova explosions from first stars kept much of the gas from forming stars
Leftover gas settled into spinning disk
Conservation of angular momentum

11. But why do some galaxies end up looking so different?
NGC 4414
M87
But why do some galaxies end up looking so different?

12. Why do galaxies differ?

13. Why don’t all galaxies have similar disks?

14. Conditions in Protogalactic Cloud?
Spin: Initial angular momentum of protogalactic cloud could determine size of resulting disk

15. Conditions in Protogalactic Cloud?
Density: Elliptical galaxies could come from dense protogalactic clouds that were able to cool and form stars before gas settled into a disk
Elliptical vs. Spiral Galaxy Formation

16. Start with the Mildly Active or Peculiar Galaxies
STARBURST galaxies 's of stars forming per year, but spread over some 100's of parsecs.
Other PECULIAR galaxies involve collisions or mergers between galaxies.
Sometimes produce strong spiral structure (e.g. M51, the "Whirlpool")
Sometimes leave long tidal tails (e.g. the "Antennae" galaxies)
Sometimes leave "ring" galaxy structures--an E passing through a S.
Sometimes see shells of stars around Es

17. Peculiar Galaxies: Starburst (NGC 7742) , Whirlpool (M51), Antennae (NGC 4038/9) in IR, Ring (AM )

18. Colliding Galaxies “Cartwheel” ring galaxy
Antennae, w/ starbursts and a simulation: a collision in progress
Collision Simulation Movie

19. Collisions may explain why elliptical galaxies tend to be found where galaxies are closer together
Stat here on 4/14

20. Giant elliptical galaxies at the centers of clusters seem to have consumed a number of smaller galaxies

21. Starburst galaxies are forming stars so quickly they would use up all their gas in less than a billion years

22. 4 MAIN CLASSES of AGN Radio Galaxies Quasars Seyfert Galaxies
BL Lacertae Objects (or Blazars with some Quasars and some Radio Galaxies)
All are characterized by central regions with NON-THERMAL radiation dominating over stellar (thermal) emission

23. Thermal vs. Non-Thermal Spectra. Normal mostly from stars,
Thermal vs. Non-Thermal Spectra Normal mostly from stars, Active mostly synchrotron

24. RADIO GALAXIES All are in Elliptical galaxies
Two oppositely directed JETS emerge from the galactic nucleus
They often feed HOT-SPOTS and and LOBES on either side of the galaxy
Radio source sizes often 300 kpc or more --- much bigger than their host galaxies.
Head-tail radio galaxies arise when jets are bent by the ram-pressure of gas as the host galaxy moves through it.
For powerful sources only one jet is seen: this is because of RELATIVISTIC DOPPER BOOSTING: the approaching jet appears MUCH brighter than an intrinsically equal receding jet since moving so FAST;
Can yield CORE DOMINATED RGs

25. Radio Galaxy: Centaurus A

26. Cygnus A and M87 Jet

27. Radio Lobes Dwarf Big Galaxy

28. Core Dominated RG (M86)

29. QUASAR PROPERTIES
QUASI-STELLAR-OBJECT: (QSO): i.e., it looks like a STAR BUT: NON-THERMAL SPECTRUM UV excess (not like a star)
BROAD EMISSION LINES  Rapid motions
VERY HIGH REDSHIFTS  not a star, but FAR away. The current (2008) convincing record redshift is z = 6.4, i.e., light emitted in FAR UV at 100 nm is received by us in the near IR at 740 nm!
HUGE DISTANCES  VERY LUMINOUS

30. NEWER QUASAR DISCOVERIES
Only about 10% are RADIO LOUD
Most show some VARIABILITY in POWER
OVV (Optically Violently Variable) QUASARS change brightness by 50% or more in a year and are highly polarized
QUASARS are AGN: surrounding galaxies detected, though small nucleus emits times MORE light than 1011 stars! “Brighter than a TRILLION suns”

31. Quasar 3C 273
Radio loud
Rare OPTICAL jet, but otherwise looks like a star
Relatively nearby quasar

32. Redshifted Spectrum of 3C 273

33. Typical Quasar Appearance
Most are actually very faint
BUT their huge redshifts imply they are billions of light-years away and intrinsically POWERFUL
Start here on 11/12

34. Radio Loud Quasar, 3C 175

35. Thought Question
What can you conclude from the fact that quasars usually have very large redshifts?
A. They are generally very distant
B. They were more common early in time
C. Galaxy collisions might turn them on
D. Nearby galaxies might hold dead quasars

36. Thought Question
What can you conclude from the fact that quasars usually have very large redshifts?
A. They are generally very distant
B. They were more common early in time
C. Galaxy collisions might turn them on
D. Nearby galaxies might hold dead quasars
All of the above!

37. Birth of a Quasar Movie Fast variability implies small size
Immense powers emerging from a volume similar to the solar system!

38. SEYFERT GALAXIES Sa, Sb galaxies with BRIGHT, SEMI-STELLAR NUCLEI
NON-THERMAL & STRONG EMISSION LINES
VARIABLE in < 1 yr  COMPACT CORE
Type 1: Broad Emission lines (like QSOs), strong in X-rays
Type 2: Only narrow Emission lines, weak in X-rays
About 1% of all Spirals are SEYFERTS, so
Either 1% of all S's are always Seyferts OR
100% of S's are Seyferts for about 1% of the time (MORE LIKELY)
OR 10% of S's are Seyferts for about 10% of the time (or any other combination of fraction and lifetime)
Start here on 11/29 and 11/30

39. A Seyfert and X-ray Variability
Circinus, only 4 Mpc away; 3C 84

40. More About Seyferts Seyferts are weak radio emitters.
CONCLUSIONS ABOUT SEYFERTS Fundamentally, they are WEAKER QSOs
Type 1: we see the center more directly Type 2: dusty gas torus blocks view of the center

41. BL Lacertae Objects
NON-THERMAL SPECTRUM: Radio through X-ray (and gamma-ray)
Radiation strongly POLARIZED
HIGHLY VARIABLE in ALL BANDS
But (when discovered) NO REDSHIFT, so distances unknown
Later, surrounding ELLIPTICAL galaxies found
CONCLUSION: greatly enhanced emission from the AGN due to RELATIVISTIC BOOSTING of a JET pointing very close to us.
BL Lacs + OPTICALLY VIOLENTLY VARIABLE QUASARS ARE OFTEN CALLED BLAZARS

42. AGN CONTAIN SUPERMASSIVE BLACK HOLES (SMBHs)
KEY LONGSTANDING ARGUMENTS:
ENERGETICS: Powers up to 1048 erg/s (1041W) Even at 100% efficiency would demand conversion of about 18 M /yr (=Mdot) into energy.
Nuclear processes produce < 1% efficiency.
GRAVIATIONAL ENERGY via ACCRETION can produce between 6% (non-rotating BH) and 32% (fastest-rotating BH),and the Luminosity is
L = G MBH Mdot / R,
with R the main distance from the Super Massive Black Hole (SMBH) where mass is converted to energy.

43. Time Variability tVAR = R / c tVAR = 104 s  R = 3 x 1014 cm = 10-4 pc
For L = 1047 erg/s,
M_dot = 10 M /yr we get MBH = 3 x 108 M and RS = 9 x 1013 cm
So, R = 3 RS
MUTUALLY CONSISTENT POWERS AND TIMESCALES.

44. RECENT OBSERVATIONAL SUPPORT
The Hubble Space Telescope has revealed that star velocities rise to very high values close to center of many galaxies and gas is orbiting rapidly, e.g. M87
Disks have been seen via MASERS in some nearby Seyfert AGN.
VLBI: radio jets formed within 1 pc of center.
There are several other more technical lines of evidence also supporting the SMBH hypothesis for AGN.

45. Rapidly Rotating Gas in M87 Nucleus
M87 zoom toward black hole

46. Direct Evidence for Rotating Disk
Masers formed in warped disk in NGC 4258 (and a few other Seyfert galaxies)

47. Evidence for Supermassive Black Holes
NGC 4261: at core of radio emitting jets is a clear disk
~300 light-yrs across and knot of emission near BH

48. SMBH Model for AGN

49. UNIFIED MODELS FOR AGN
Three main parameters: MBH; the accretion rate, M_dot, and viewing angle to the accretion disk axis, 
Main ingredients:
SMBH > 106 M
10-5 pc < accretion disk < 10-1 pc (AD)
broad line clouds < 1 pc (BLR)
thick, dusty, torus < 100 pc
narrow line clouds < 1000 pc (NLR)
sometimes, a JET (usually seen from < 102 pc to maybe 106 pc!)
Start here on 4/16

50. Unification for Radio Quiet and Radio Loud
High MBH, M_dot:
 small: QSO is seen including AD and BLR
 large: only NLR plus radiating torus: seen as UltraLuminous InfraRed Galaxies (ULIRGs)
Low MBH, M_dot:
 small: Seyfert Type 1  big: Seyfert Type 2
RADIO LOUD (Jets)
High MBH, M_dot:
 very small: Optically Violently Variable Quasar
 small: radio loud quasar (QSR)
 large: classical double radio galaxy (FR II type)
Low MBH. M_dot:
 very small: BL Lac object
 small: broad line radio galaxy (FR I type)
 large: narrow line radio galaxy

51. Different AGN from Different Angles
Luminous: Quasars seen close to perpendicular to disk and Ultraluminous Infrared Galaxies near disk plane
Weaker: Type 1 or Type 2 Seyferts
If jets are important:
BL Lacs along jet axis,
Quasars at modest angles & Radio Galaxies at larger angles

52. Black Holes in Galaxies
Many nearby galaxies – perhaps all of them – have supermassive black holes at their centers
These black holes seem to be dormant active galactic nuclei
All galaxies may have passed through a quasar-like stage earlier in time

53. Galaxies and Black Holes
Mass of a galaxy’s central black hole is closely related to mass of its bulge